Evolutionary tracks in the Hertzsprung-Russell diagrams. Non-rotating models are shown in the panels in the left column. The plain lines in the panels of the middle and right column are the rotating models with a moderate angular momentum transport. The dashed lines are the models computed with a strong angular momentum transport. We note that at low rotations (υ/υ_crit = 0.2), models with moderate and strong angular momentum transport may overlap nearly exactly preventing to see the dashed lines (see e.g., the 7 M_⊙ stellar model). The shaded area shows the instability strip (determined as in Anderson et al. 2016). The models were computed up to MS turnoff for most stars, the lowest mass stars were expended up to the end of He-burning. In the bottom right panel, the parts of the tracks where the mass fraction of hydrogen at the surface is below 0.4, meaning the star may be considered a Wolf-Rayet, are highlighted by a broad blue band.